XX Perseus ( IRC +50052 / HIP 9582 / BD + 54 444 , XX Persei ) is a semi - regular variable star , a red supergiant in the Perseus constellation between the Double Cluster and the border with the Andromeda constellation .
| XX Perseus | |||
|---|---|---|---|
| Star | |||
| Observational data ( Age J2000.0 ) | |||
| Right ascension | |||
| Declination | |||
| Distance | 2290 [2] | ||
| Visible magnitude ( V ) | 7.9 - 9.0 [3] | ||
| Constellation | Perseus | ||
| Astrometry | |||
| Radial velocity ( R v ) | and | ||
| Own movement (μ) | RA: -1.213 ± 0.039 [6] Dec: -1.543 ± 0.036 [6] | ||
| Parallax (π) | 0.95 ± 0.46 [6] mas | ||
| Absolute magnitude (V) | −4.6 [7] | ||
| Characteristics | |||
| Spectral class | M4Ib + B7V [8] | ||
| Variability | SRc [9] | ||
| physical characteristics | |||
| Weight | 16 [7] M ☉ | ||
| Radius | 710 R ☉ | ||
| Temperature | 3700 [10] K | ||
| Luminosity | 85000 [10] L ☉ | ||
| |||
| Database Information | |||
| SIMBAD | data | ||
Content
- 1 Variability
- 2 distance
- 3 Properties
- 4 Companion
- 5 notes
Variability
XX Perseus is a semi-regular variable star of the SRc subtype, that is, it is a cold supergiant. The general catalog of variable stars indicates a period of 415 days. [9] A larger second period is also indicated, with an initial estimate of 4,100 days. [7] A more modern study showed only slow changes with a period of 3150 ± 1000 days. [3] In another study, no long periods of up to 10,000 days were found. [eleven]
Distance
The most probable estimate of the distance to XX Perseus is 2290 pc , since it is believed that the star belongs to the OB1 Perseus association. [2]
Properties
XX Perseus is a red supergiant of the spectral class M4Ib with an effective temperature of 3700 K. The star has a large infrared excess, which indicates the presence of dust with a temperature of 900 K. No maser radiation sources were detected. [10] [12]
XX Perseus has a mass of 16 solar masses , which exceeds the value starting from which supernova explosions are possible. [7]
Companion
XX Perseus possesses a companion of magnitude 9.7 at an angular distance of 20.5 ". [8] The spectral class of the binary system has the form M4Ib + B7V, [8] but the ultraviolet spectrum of the companion star indicates spectral class A. [13]
Notes
- ↑ 1 2 F .; Van Leeuwen. Validation of the new Hipparcos reduction // Astronomy and Astrophysics . - EDP Sciences 2007. - Vol. 474 , no. 2 . - P. 653 . - DOI : 10.1051 / 0004-6361: 20078357 . - . - arXiv : 0708.1752 .
- ↑ 1 2 Megan; Reiter Marengo, Massimo; Hora, Joseph L .; Fazio, Giovanni G. A Spitzer / IRAC characterization of Galactic AGB and RSG stars // Monthly Notices of the Royal Astronomical Society : journal. - Oxford University Press , 2015. - Vol. 447 , no. 4 . - P. 3909 . - DOI : 10.1093 / mnras / stu2725 . - . - arXiv : 1501.02749 .
- ↑ 1 2 LL; Kiss; Szabó, Gy. M .; Bedding, TR . Variability in red supergiant stars: Pulsations, long secondary periods and convection noise (Engl.) // Monthly Notices of the Royal Astronomical Society : journal. - Oxford University Press , 2006. - Vol. 372 , no. 4 . - P. 1721 . - DOI : 10.1111 / j.1365-2966.2006.10973.x . - . - arXiv : astro-ph / 0608438 .
- ↑ 1 2 3 4 B. Famaey , X. Luri Local kinematics of K and Miants from CORAVEL / Hipparcos / Tycho-2 data // Astron. Astrophys. - EDP Sciences , 2005. - Vol. 430, Iss. 1. - P. 165–186. - ISSN 0004-6361 ; 0365-0138 ; 1432-0746 ; 1286-4846 - doi: 10.1051 / 0004-6361: 20041272
- ↑ 1 2 3 4 Collaboration G. Gaia DR2 - 2018 .-- T. 1345. - P. 0.
- ↑ 1 2 3 Gaia Collaboration. VizieR Online Data Catalog: Gaia DR1 (Gaia Collaboration, 2016) (Italian) // VizieR On-line Data Catalog: I / 337. Originally published in: Astron. Astrophys: diario. - 2016 .-- V. 1337 . - .
- ↑ 1 2 3 4 R .; Stothers; Leung, KC Luminosities, masses and periodicities of massive red supergiants (Eng.) // Astronomy and Astrophysics : journal. - EDP Sciences 1971. - Vol. 10 . - P. 290 . - .
- ↑ 1 2 3 D .; Proust; Ochsenbein, F .; Pettersen, BR A catalog of variable-visual binary stars (Eng.) // Astronomy and Astrophysics Supplement Series . - EDP Sciences , 1981. - Vol. 44 . - P. 179 . - .
- ↑ 1 2 NN; Samus; Durlevich, OV et al. VizieR Online Data Catalog: General Catalog of Variable Stars (Samus + 2007-2013) (Eng.) // VizieR On-line Data Catalog: B / gcvs. Originally published in: 2009yCat .... 102025S: journal. - 2009. - Vol. 1 . - .
- ↑ 1 2 3 Thomas KT; Fok; Nakashima, Jun-Ichi; Yung, Bosco HK; Hsia, Chih-Hao; Deguchi, Shuji. Maser Observations of Westerlund 1 and Comprehensive Considerations on Maser Properties of Red Supergiants Associated with Massive Clusters // The Astrophysical Journal : journal. - IOP Publishing 2012. - Vol. 760 . - P. 65 . - DOI : 10.1088 / 0004-637X / 760/1/65 . - . - arXiv : 1209.6427 .
- ↑ John R .; Percy; Sato, Hiromitsu. Long Secondary Periods in Pulsating Red Supergiant Stars (English) // Journal of the Royal Astronomical Society of Canada: journal. - 2009. - Vol. 103 . - P. 11 . - .
- ↑ L .; Verheyen; Messineo, M .; Menten, KM SiO maser emission from red supergiants across the Galaxy. I. Targets in massive star clusters (Eng.) // Astronomy and Astrophysics : journal. - EDP Sciences 2012. - Vol. 541 . - P. A36 . - DOI : 10.1051 / 0004-6361 / 201118265 . - . - arXiv : 1203.4727 .
- ↑ Richard H .; Buss; Snow, Theodore P. Hot components and circumstellar grains in M supergiant syncretic binaries (Eng.) // The Astrophysical Journal : journal. - IOP Publishing 1988. - Vol. 335 . - P. 331 . - DOI : 10.1086 / 166931 . - .